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Question: In Ex. 11.3 we assumed the velocity and acceleration were (instantaneously,

at least) collinear. Carry out the same analysis for the case where they are

perpendicular. Choose your axes so that v lies along the z axis and a along the x axis

(Fig. 11.14), so thatv=vz^,a=ax^,andr^=²õ¾±²Ô賦´Ç²õÏ•x^+sinv=vz^,a=ax^,andr^=²õ¾±²Ô賦´Ç²õÏ•x^+sinsinÏ•y^+³¦´Ç²õθz^Check that P is consistent with the Lienard formula.

dP»åΩ=μ0q2a216Ï€2c1-⳦´Ç²õθ2-1-β2sin2賦´Ç²õ2Ï•1-⳦´Ç²õθ5,P=μ0q2a2γ46Ï€³¦[Answer: .For relativistic velocities ( β≈1) the radiation is again sharply peaked in the forward

direction (Fig. 11.15). The most important application of these formulas is to circular motion-in this case the radiation is called synchrotron radiation. For a relativistic electron, the radiation sweeps around like a locomotive's headlight as the particle moves.]

Short Answer

Expert verified

Answer

The Lienard formula is

dP»åΩ=μ0q2a216Ï€2c1-⳦´Ç²õθ2-1-β2sin2賦´Ç²õ2Ï•1-⳦´Ç²õθ5,P=μ0q2a2γ46Ï€³¦

and the power found by integrating and the distribution agree to each other.

Step by step solution

01

Determine the formula:

Consider the formula for the angular distribution of the power as:

dP»åΩ=q216Ï€2ε0r^×u×a2r^·u5

Here, the terms are:

u=xr^-vz^a=ax^r^=sinθcosϕx^+sinsinϕy^+cosθz^\

Determine the terms in the second fraction as:

dr^·u=c-vcosθ=c1-βcosθ …. (1)

Solve further as:

r^×u×a2=ur^·a-ar^·u2r^×u×a2=uasinθcosϕ-ac1-βcosθx^2r^×u×a2=a2c21-βcosθ2-1-βsin2θcos2ϕ …… (2)

02

Determine if P is consistent with the Lienard formula:

From equation (1) and (2) determine the formula for the angular power as:

dPdΩ=q216π2ε0a2c21-βcosθ2-1-β2sin2θcos2ϕc31-βcosθ5dPdΩ=μ0q2a216π2c1-βcosθ2-1-β2sin2θcos2ϕ1-βcosθ5μ0ε0=1c2

In order to determine the total power integrate over the space angle

dΩ=dθsinθϕasfollowsP=μ0q2a216π2c∫02π∫0π1-βcosθ2-1-β2sin2θcos2ϕ1-βcosθ5sinθdθdϕ

Using ∫02πcos2ϕ=πintegrate over as follows:

P=μ0q2a216π2c∫0π21-βcosθ2-1-β2sin2θ1-βcosθ5sinθdθ=μ0q2a216π2cJ

Solve for the integral J as follows:

J=∫1-β1+β2u2-1-β21-1-2u+u2β21-βcosθ5sinθdθ1-βcosθ=u,sin2θ=1-1-2u+u2β2,\hfilldu=βsinθdθ=1β3-1-β2214u4+21-β213u3-1+β212u21+β1+β

Solve for the terms in the bracket as:

First term:

-1+β212u21+β1+β=-1+β22-4β1-β21+β2=2β1+β21-β22

Second term:

21-β213u31+β1+β=231-β2-6β-2β31-β31+β3=4β3+β231-β22

Third term:

-1-β214u41+β1+β=1-β248β+8β31-β41+β4=2β1+β2β1-β22

Rewrite the integral as:

J=131-β2221+β2β-43β3+β2+2β2+β2=831-β22=83γ4γ=1-β2-12

Therefore, the expression for the power is written as:

P=μ0q2a216πc83γ4=μ0q2a26πcγ4 ….. (3)

From the Lienard formula solve as:

P=μ0q2γ66πca2-v×ac2=μ0q2γ66πca2-a2β2v×a=va=μ0q2a26πcγ4P=μ0q2γ66πca2-v×ac2=μ0q2γ66πca2-a2β2v×a=va=μ0q2a26πcγ4 …… (4)

Since, the velocity and acceleration are perpendicular to each other so the equation (3) and (4) agrees:

Therefore, the Lienard formula is

dPdΩ=μ0q2a216π2c1-βcosθ2-1-β2sin2θcos2ϕ1-βcosθ5

and the power found by integrating and the distribution agree to each other.

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Most popular questions from this chapter

As you know, the magnetic north pole of the earth does not coincide with the geographic north pole—in fact, it’s off by about 11°. Relative to the fixed axis of rotation, therefore, the magnetic dipole moment of the earth is changing with time, and the earth must be giving off magnetic dipole radiation.

(a) Find the formula for the total power radiated, in terms of the following parameters:ψ (the angle between the geographic and magnetic north poles), M (the magnitude of the earth’s magnetic dipole moment), andӬ (the angular velocity of rotation of the earth). [Hint: refer to Prob. 11.4 or Prob. 11.11.]

(b) Using the fact that the earth’s magnetic field is about half a gauss at the equator, estimate the magnetic dipole moment Mof the earth.

(c) Find the power radiated. [Answer: 4×10-5W]

(d) Pulsars are thought to be rotating neutron stars, with a typical radius of 10 km, a rotational period of 10-3s, and a surface magnetic field of 108T. What sort of radiated power would you expect from such a star? [Answer: 2×1036W].

An electric dipole rotates at constant angular velocity Ӭin thexy plane. (The charges,±q , are at r±=±R(cosӬtx^+sinӬty^); the magnitude of the dipole moment is p=2qR.)

(a) Find the interaction term in the self-torque (analogous to Eq. 11.99). Assume the motion is nonrelativistic ( Ó¬R<<c).

(b) Use the method of Prob. 11.20(a) to obtain the total radiation reaction torque on this system. [answer: -μ0p2Ó¬36Ï€³¦z^]

(c) Check that this result is consistent with the power radiated (Eq. 11.60).

In Bohr’s theory of hydrogen, the electron in its ground state was supposed to travel in a circle of radius 5×10-11m, held in orbit by the Coulomb attraction of the proton. According to classical electrodynamics, this electron should radiate, and hence spiral in to the nucleus. Show thatv≪c for most of the trip (so you can use the Larmor formula), and calculate the lifespan of Bohr’s atom. (Assume each revolution is essentially circular.)

Check that the retarded potentials of an oscillating dipole (Eqs. 11.12 and 11.17) satisfy the Lorenz gauge condition. Do not use approximation 3.

(a) A particle of charge qmoves in a circle of radiusRat a constant speedv. To sustain the motion, you must, of course, provide a centripetal forcemv2Rwhat additional force (Fe) must you exert, in order to counteract the radiation reaction? [It's easiest to express the answer in terms of the instantaneous velocityv.] What power (Pe) does this extra force deliver? ComparePewith the power radiated (use the Larmor formula).

(b) Repeat part (a) for a particle in simple harmonic motion with amplitudeand angular frequency:Ӭ.Ӭ(t)=Acos(Ӭt)z⌢ Explain the discrepancy.

(c) Consider the case of a particle in free fall (constant accelerationg). What is the radiation reaction force? What is the power radiated? Comment on these results.

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